After inflation ends, we must recover a radiation dominated universe before Big Bang Nucleosynthesis (BBN), made of minimum the Standard Model particles. This period when the inflaton energy density is transferred to the thermal bath is called reheating [1]}, [2]}, [3]}, and requires the interaction of the inflaton field with other particle species. But even before reheating, interactions can lead to dissipative effects during inflation, and the continuous transfer of inflaton energy density into radiation. In the context of slow-roll inflation, this is modelled by the introduction of an additional friction term, the dissipative coefficient \(\Upsilon \) , in the inflaton \(\phi \)  equation of motion (eom):
\(\ddot{\phi }+ (3 H + \Upsilon ) \dot{\phi }+ V_\phi =0 \,,\) 
